GW170817, general relativistic magnetohydrodynamic simulations, and the neutron star maximum mass

Ruiz, Milton; Shapiro, Stuart L.; Tsokaros, Antonios

doi:10.1103/physrevd.97.021501

Cited by 495 publications

(468 citation statements)

References 85 publications

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“…Combining these results one therefore obtains that M TOV < 2.2 M . This simple estimate is in agreement with the results of References [52,54,55] and it again disfavors very stiff equations of state which predict maximum masses above 2.2 M such as e.g., DD2 [56].…”

Section: Analysis Of the Gw Signalsupporting

confidence: 89%

The Merger of Two Compact Stars: A Tool for Dense Matter Nuclear Physics

et al. 2018

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Abstract:We discuss the different signals, in gravitational and electromagnetic waves, emitted during the merger of two compact stars. We will focus in particular on the possible contraints that those signals can provide on the equation of state of dense matter. Indeed, the stiffness of the equation of state and the particle composition of the merging compact stars strongly affect, e.g., the life time of the post-merger remnant and its gravitational wave signal, the emission of the short gamma-ray-burst, the amount of ejected mass and the related kilonova. The first detection of gravitational waves from the merger of two compact stars in August 2017, GW170817, and the subsequent detections of its electromagnetic counterparts, GRB170817A and AT2017gfo, is the first example of the era of "multi-messenger astronomy": we discuss what we have learned from this detection on the equation of state of compact stars and we provide a tentative interpretation of this event, within the two families scenario, as being due to the merger of a hadronic star with a quark star.

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Section: Analysis Of the Gw Signalsupporting

confidence: 89%

The Merger of Two Compact Stars: A Tool for Dense Matter Nuclear Physics

et al. 2018

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“…These multimessenger signals have been used to impose some constraints on the physical properties of a neutron star (see e.g. [10,43,[91][92][93][94][95][96][97] and references therein), such as the maximum mass of a spherical star, tidal deformability, equation of state, radius of a neutron star, etc.…”

Section: Discussionmentioning

confidence: 99%

Magnetohydrodynamic simulations of binary neutron star mergers in general relativity: Effects of magnetic field orientation on jet launching

2020

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Binary neutron star mergers can be sources of gravitational waves coincident with electromagnetic counterpart emission across the spectrum. To solidify their role as multimessenger sources, we present fully 3D, general relativistic, magnetohydrodynamic simulations of highly spinning binary neutrons stars initially on quasicircular orbits that merge and undergo delayed collapse to a black hole. The binaries consist of two identical stars modeled as Γ = 2 polytropes with spin χNS = 0.36 aligned along the direction of the total orbital angular momentum L. Each star is initially threaded by a dynamical unimportant interior dipole magnetic field. The field is extended into the exterior where a nearly force-free magnetosphere resembles that of a pulsar. The magnetic dipole moment µ is either aligned or perpendicular to L and has the same initial magnitude for each orientation. For comparison, we also impose symmetry across the orbital plane in one case where µ in both stars is aligned along L. We find that the lifetime of the transient hypermassive neutron star remnant, the jet launching time, and the ejecta (which can give rise to a detectable kilonova) are very sensitive to the magnetic field orientation. By contrast, the physical properties of the black hole + disk remnant, such as the mass and spin of the black hole, the accretion rate, and the electromagnetic (Poynting) luminosity, are roughly independent of the initial magnetic field orientation. In addition, we find imposing symmetry across the orbital plane does not play a significant role in the final outcome of the mergers. Our results suggest that, as in the black hole-neutron star merger scenario, an incipient jet emerges only when the seed magnetic field has a sufficiently large-scale poloidal component aligned to the initial orbital angular momentum. The lifetime [∆t 140(MNS/1.625M )ms] and Poynting luminosities [LEM 10 52 erg/s] of the jet, when it forms, are consistent with typical short gamma ray bursts, as well as with the Blandford-Znajek mechanism for launching jets.

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“…[10]), the constraint would further tighten to Rð1.4 M ⊙ Þ < 12.5 km. We note that this maximalradius constraint is unaffected by the proposed limit of M max < 2.16 M ⊙ [25][26][27], stemming from the resulting kilonova observations associated with the GW170817 event [10,[28][29][30][31][32][33][34][35]. This is because, for a given radius, there are many EOSs whose maximal mass is smaller than that of the EOS with the highest maximal mass.…”

mentioning

confidence: 92%

“…Also in this figure, we display black dashed lines to indicate where the upper and lower edges become truncated with a further restriction of M max < 2.16 M ⊙ , a bound proposed in Refs. [25][26][27] stemming from the resulting kilonova observations associated with GW170817.…”

Section: Tropesmentioning

confidence: 99%

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Gravitational-Wave Constraints on the Neutron-Star-Matter Equation of State

et al. 2018

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The detection of gravitational waves originating from a neutron-star merger, GW170817, by the LIGO and Virgo Collaborations has recently provided new stringent limits on the tidal deformabilities of the stars involved in the collision. Combining this measurement with the existence of two-solar-mass stars, we generate a generic family of neutron-star-matter equations of state (EOSs) that interpolate between state-ofthe-art theoretical results at low and high baryon density. Comparing the results to ones obtained without the tidal-deformability constraint, we witness a dramatic reduction in the family of allowed EOSs. Based on our analysis, we conclude that the maximal radius of a 1.4-solar-mass neutron star is 13.6 km, and that the smallest allowed tidal deformability of a similar-mass star is Λð1.4 M ⊙ Þ ¼ 120.

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GW170817, general relativistic magnetohydrodynamic simulations, and the neutron star maximum mass

Cited by 495 publications

References 85 publications

The Merger of Two Compact Stars: A Tool for Dense Matter Nuclear Physics

The Merger of Two Compact Stars: A Tool for Dense Matter Nuclear Physics

Magnetohydrodynamic simulations of binary neutron star mergers in general relativity: Effects of magnetic field orientation on jet launching

Gravitational-Wave Constraints on the Neutron-Star-Matter Equation of State

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